The first two rows of Figure REF  display the relative drop in the flux \(\Delta F\)  across the accretion flow
for the SpherAcc and Polar geometries.
The drop is mainly an increasing function of \(\dot{M}/f_{\mathrm {fill}}\)  and ranges between \(\Delta F=0~\%\)  (no absorption)
and nearly \(\Delta F=100\)  % over the parameter space considered.
Already for \(\dot{M} \approx 3\times 10^{-5}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\) , there is noticeable absorption
with \(\Delta F\approx 20\) –50 % depending on the mass, with more absorption at lower planet masses.
This corresponds to an extinction \(A_R\approx 2\) –4 mag.
The increase of extinction with decreasing planet mass (and thus, at a given \(\dot{M} \) , with the gas column density) can be seen from
Equation (REF ).
Also, for the three highest \(\dot{M} \)  values in Figure REF , the opacity increases with decreasing temperature (due to the contribution from water; [1]}) and increasing density, that is, decreasing mass.
For moderate \(\dot{M} \lesssim 10^{-5}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\) , the extinction is at most \(A_R\approx 0.5\)  mag.
